Issue |
A&A
Volume 440, Number 3, September IV 2005
|
|
---|---|---|
Page(s) | 791 - 797 | |
Section | Cosmology (including clusters of galaxies) | |
DOI | https://doi.org/10.1051/0004-6361:20053139 | |
Published online | 05 September 2005 |
The quiescent Hubble flow, local dark
energy tests, and pairwise velocity dispersion in a
universe
1
Tuorla Observatory, University of Turku, 21500 Piikkiö, Finland e-mail: pekkatee@utu.fi
2
Division of Astronomy, University of Oulu, 90014, Finland
3
Sternberg Astronomical Institute, Moscow University, 119899 Moscow, Russia
4
Institute of Astronomy, St. Petersburg State University, Staryj Peterhoff, 198504 St. Petersburg, Russia
5
Isaac Newton Institute of Chile, Saint-Petersburg Branch, Russia
Received:
24
March
2005
Accepted:
10
May
2005
We review the increasing evidence for the cosmological relevance
of the cold local Hubble flow. New observations, N-body
simulations and other theoretical arguments
are discussed, supporting our previous suggestion that the
cosmological vacuum or uniform dark energy can have locally observable
consequencies, especially a lower velocity scatter in DE dominated
regions.
The apparent contradiction between the slight dependence
of the growth factor on and the significant influence
of dark energy in realistic N-body calculations is clarified.
An interesting new result is
that in the standard Λ cosmology, gravitation
dominates
around a typical matter fluctuation up to about the correlation
length r0, and we tentatively link this with the high pairwise velocity
dispersion
on scales up to several Mpc, as measured from galaxy redshift-space
correlations.
Locally, the smooth Hubble flow on similar scales is consistent with
N-body simulations including
and a low
density contrast in the Local Volume, which make it generally
vacuum-dominated beyond
Mpc from galaxies and groups.
We introduce a useful way to view the Hubble flow in terms of
“zero gravity” spheres
around galaxies: e.g., a set of non-intersecting spheres, observed to be
expanding, actually participates in accelerating expansion.
The observed insensitiveness of the local velocity dispersion to
galaxy mass is explained as an effect of the vacuum, too.
Key words: dark matter / cosmological parameters / Local Group
© ESO, 2005
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